Other
Scientific paper
Sep 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006dps....38.0403k&link_type=abstract
American Astronomical Society, DPS meeting #38, #04.03; Bulletin of the American Astronomical Society, Vol. 38, p.487
Other
Scientific paper
Some debris disks, exemplified by epsilon Eridani, show azimuthal substructure ("clumps"), which may stem from resonances with as yet undetected planets. There are two basic ways in which planets can make debris disks clumpy. In one scenario, the Poynting-Robertson force is responsible for dust delivery from outer regions of the disk to locations of external mean-motion planetary resonances; the captured particles form characteristic clumps. In another scenario, a population of planetesimals, locked in a resonance with the planet ("trojans", "plutinos"), produces dust which stays in the same resonance, creating the observed clumps. We have constructed simple analytic models to investigate the efficiency of both scenarios for a wide range of stars, planets, disk densities, and planetesimal families. We find that the first scenario works well only in very tenuous disks. At the optical depth level of all debris disks resolved so far, the first scenario would generate a narrow resonant ring with hardly visible azimuthal structure, rather than clumps. The efficiency of this scenario depends on stellar luminosity, planet's mass and its orbital radius only weakly. The efficiency of the second scenario is proportional to the mass of the resonant planetesimal family. A family of roughly martian or even lunar mass could be sufficient to account for the clumps observed in the epsilon Eridani disk. The brightness of the clumps produced by the second scenario increases with decreasing luminosity of the star, increasing planetary mass, and decreasing orbital radius of the planet. The model of the second scenario is more uncertain than that of the first one, because it depends quite sensitively on poorly known properties of the collisional grinding process. The same idea of the two scenarios may apply to other kinds of structures (gaps, rings, etc.) as well.
Krivov Alexander
Löhne Torsten
Miodrag Sremčević
Queck Martina
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